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Table 2.

Spectroscopic, sample-selection, and structural characteristics of the INSPIRE DR1 sample.

ID Sample zXSH zprev M⋆ ⟨Re⟩ ⟨Re⟩ Re, r Re, r nr qr R50UVB R50VIS
KiDS (1011 M⊙) (″) (kpc) (″) (kpc) (″) (″)
J0211–3155 T18 0.3012 0.30135 0.876 0.237 1.07 0.237 1.07 8.1 0.48 0.58 0.55
J0224–3143 T18 0.3839 0.3853 2.710 0.292 1.55 0.247 1.31 6.1 0.39 0.55 0.55
J0226–3158 T18 0.2355 0.2364 0.688 0.350 1.32 0.337 1.27 3.7 0.60 0.58 0.50
J0240–3141 T18 0.2789 0.2809 0.981 0.189 0.81 0.189 0.81 8.1 0.27 0.60 0.50
J0314–3215 T18 0.2874 0.2888 1.000 0.150 0.66 0.148 0.65 5.5 0.39 0.55 0.50
J0316–2953 T18 0.3596 0.3102 0.873 0.200 1.02 0.200 1.02 3.5 0.31 0.58 0.50
J0317–2957 T18 0.2611 0.2610 0.873 0.257 1.05 0.257 1.05 5.0 0.21 0.59 0.50
J0321–3213 T18 0.2947 0.2953 1.233 0.309 1.37 0.281 1.25 4.9 0.39 0.60 0.50
J0326–3303 T18 0.2971 0.2976 0.930 0.321 1.44 0.321 1.44 3.7 0.35 0.60 0.50
J0838+0052 S20 0.2702 0.2703 0.870 0.306 1.28 0.351 1.47 4.0 0.41 0.55 0.50
J0842+0059 S20 0.2959 0.2946 0.910 0.226 1.01 0.226 1.01 3.3 0.29 0.55 0.50
J0847+0112 (*) T18 0.1764 0.17636 0.989 0.456 1.37 0.465 1.40 3.3 0.26 0.60 0.55
J0857–0108 S20 0.2694 0.2696 1.000 0.336 1.40 0.366 1.53 2.9 0.33 0.60 0.55
J0918+0122 T18 0.3731 0.3733 2.263 0.328 1.71 0.328 1.71 6.0 0.51 0.60 0.55
J0920+0212 (*) T18 0.2800 0.2797 1.031 0.345 1.48 0.345 1.48 2.0 0.32 0.58 0.55
J2305–3436 T18 0.2978 0.30146 0.857 0.307 1.29 0.293 1.23 3.4 0.40 0.55 0.50
J2312–3438 T18 0.3665 0.3664 1.344 0.243 1.25 0.243 1.25 2.3 0.43 0.60 0.60
J2327–3312 T18 0.4065 0.40661 1.569 0.276 1.15 0.276 1.51 5.9 0.67 0.58 0.50
J2359–3320 T18 0.2885 0.28922 1.065 0.237 1.03 0.237 1.04 4.4 0.39 0.58 0.50

Notes. In the first block of columns, we provide the KiDS publication from where each candidate was taken and the new redshifts inferred from XSH spectra. The first column of the second block lists instead the previously estimated redshifts. The two values are always in fair agreement. The previous redshifts, as well as the median (gri) size and stellar masses also provided in the same block, have been used for the INSPIRE object selection. The third block lists the structural parameters presented in T18 and/or S20 and obtained from the r-band KiDS images (the image with the best seeing), which are also shown in the histograms in Fig. 3, together with stellar masses. Finally, in the last block of columns, we report the apertures that encapsulate 50% of the light for the UVB and VIS arm, respectively (see Sect. 4.1). (*)Also observed in GAMA.

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